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Light elements in stars with exoplanets

Published online by Cambridge University Press:  09 March 2010

E. Delgado Mena
Affiliation:
Instituto de Astrofísica de Canarias, E-38200 La Laguna, Tenerife, Spain. email: edm@iac.es
M. C. Gálvez-Ortiz
Affiliation:
Centre for Astrophysics Research, Science and Technology Research Institute, University of Hertfordshire, Hatfield AL10 9AB, UK.
J. I. González-Hernández
Affiliation:
Departamento de Astrofísica, Facultad de Ciencias Físicas, Universidad Complutense de Madrid, E-28040, Spain.
G. Israelian
Affiliation:
Instituto de Astrofísica de Canarias, E-38200 La Laguna, Tenerife, Spain. email: edm@iac.es
N. C. Santos
Affiliation:
Centro de Astrofísica, Universidade do Porto, Rua das Estrelas, 4150-762 Porto, Portugal. Observatoire de Genève, 51 ch. des Maillettes, CH-1290 Sauverny, Switzerland.
R. Rebolo
Affiliation:
Instituto de Astrofísica de Canarias, E-38200 La Laguna, Tenerife, Spain. email: edm@iac.es Consejo Superior de Investigaciones Científicas, E-28006, Madrid, Spain.
C. Dominguez Cerdeña
Affiliation:
Instituto de Astrofísica de Canarias, E-38200 La Laguna, Tenerife, Spain. email: edm@iac.es
Corresponding
E-mail address:
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Abstract

Light elements are important tracers of the internal stellar structure and kinematics. Li and Be are both burned in the stellar interiors but Be requires much higher temperatures and thus we can expect to measure Be abundances in stars which have no detectable Li in their atmospheres. The study of these elements can give us information about processes related to the angular momentum history of these stars, since rotation and angular momentum loss are important mechanisms responsible for the depletion of light elements. Additionally, if pollution has played an important role in determining the high-metal content of planet host stars, we would expect to find a similar or even higher increase in the Li and Be contents. We present Be and Li abundances in a sample of 69 stars with planets and 31 stars without known planetary companion, spanning a large range of effective temperatures.

Type
Contributed Papers
Copyright
Copyright © International Astronomical Union 2010

References

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